Spectral effects simulation with two-dimensional magnetohydrodynamic models of the solar photosphere

TL;DR

This study uses two-dimensional MHD models to simulate spectral effects in the solar photosphere, analyzing how magnetic flux influences spectral line profiles and comparing results with observations.

Contribution

It introduces detailed spectral simulations using 2D MHD models to understand magnetic effects on solar photospheric spectral lines.

Findings

Simulated wavelength shifts are smaller than observed.

Spectral line asymmetries vary with magnetic flux and viewing angle.

Models show good qualitative but limited quantitative agreement with observations.

Abstract

To study the structure of spatially unresolved features of the solar photosphere, we calculated the Stokes profiles of seven photospheric iron lines using two-dimensional nonstationary MHD models of solar granulation for various amounts of magnetic flux (0, 10, 20, 30 mT). We investigate variations in the absolute wavelength shifts and bisectors of the I profiles, as well as variations in the zero-crossing wavelength shifts, amplitude and area asymmetry of the V profiles as functions of magnetic field strength and time. The center-to-limb variations of the Stokes profiles are analyzed. The iron abundance is found to be 7.57, with the photosphere inhomogeneities taken into account. Although most of the spectral effects simulated within the scope of the two-dimensional MHD models are in satisfactory agreement with observational data, these models cannot always give a quantitative agreement. The absolute wavelength shifts of the Stokes profiles of Fe II lines calculated with the MHD models are substantially smaller than the observed ones.